From the perspective of a telescope system (under a Frozen Flow assumption[1]}), wind layers will present as static turbulent scenes
crossing over the telescope primary mirror at the speed of the wind at that height. Given enough data in time to adequately sample a wind velocity, these pupil crossing times
will have high signal to noise peaks across spatial Fourier modes, as different spatial scales will cross with different frequencies. Therefore, when turbulent phase screens are decomposed into Fourier modes, each coefficient
contains information on a spatial frequency of a particular size that
maps to a series of non-conflicting controllers. A PSD for each coefficient reveals
the peak frequency, height, and width for each wind layer, which provides input to a controller specific to that coefficient.
